Radial profiles of the migration-related parameters at the end of one of the simulations with r₀ = 10 au. (a) q_T remains constant in our disc model, while p_∑ varies greatly and changes sign across the pressure bump. (b) Coefficients for τ_a also change sign but at slightly different locations according to Eqs. (24) and (25), respectively. (c) τ_a near the pressure bump for embryos of different masses with e = 10⁻³ and i = e/2, where inward migration is denoted by red and outward migration is denoted by blue. The migration rate slows down and changes sign slightly interior (≈14 au) to the location of planetesimal formation (≈14.2 au). (d) τ_e at the same locations, which is ∝t_wav ∝ m⁻¹. This shows type-I damping starts to become efficient when the embryos are ≳10⁻¹ M_⊕.